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We have characterized the double red giant eclipsing binary KIC 9246715 with a combination of dynamical modeling, stellar atmosphere modeling, and global asteroseismology, and have investigated the roles of magnetic activity, tidal forces, and stellar evolution in creating the system we observe today. KIC 9246715 represents a likely future state of similar-mass RG/EB systems and raises interesting questions about the interactions among stellar activity, tides, and solar-like oscillations.  The two stars in KIC 9246715 are nearly twins ($M_1 = 2.171\substack{+0.006 \\ -0.008} \ M_{\odot}$, $M_2 = 2.149\substack{+0.006 \\ -0.008} \ M_{\odot}$, $R_1 = 8.37\substack{+0.03 \\ -0.07} \ R_{\odot}$, $R_2 = 8.30\substack{+0.04 \\ -0.03} \ R_{\odot}$), yet we find only one set of solar-like oscillations strong enough to measure robustly ($M = 2.17 \pm 0.14 \ M_{\odot}$, $R = 8.26 \pm 0.18 \ R_{\odot}$). \newrevise{The asteroseismic mass and radius agree with both Star 1 and Star 2, as does the surface gravity derived from asteroseismology ($\log g = 2.942 \pm 0.008$; compare with $\log g_1 = 2.929\substack{+0.007 \\ -0.003}$ and $\log g_2 = 2.932\substack{+0.003 \\ -0.004}$). The asteroseismic density, which is not a function of temperature, is systematically larger than Star 1 and Star 2, but is a slightly closer match with Star 2 ($\bar{\rho}_{\rm{seismic}}/\bar{\rho}_\odot = (3.86 \pm 0.02) \times 10^{-3}$; compare with $\bar{\rho}_1/\bar{\rho}_\odot = (3.70\substack{+0.10 \\ -0.04}) \times 10^{-3}$ and $\bar{\rho}_2/\bar{\rho}_\odot = (3.76\substack{+0.04 \\ -0.05}) \times 10^{-3}$). As a result, we cannot conclude which star is the source of the main oscillations from asteroseismology alone. However, Star 2 appears to be less active than Star 1, and we therefore tentatively assign the main oscillations to Star 2.} We identify a second set of marginally detectable oscillations potentially attributable to Star 1, for which only $\Delta \nu$ can be estimated, yielding a higher average density than the main oscillation spectrum. \newrevise{This is not consistent with the expected density of Star 1, however, which is less than that of Star 2. While these These  extra modescertainly exist, they  may represent a spurious detection.} Surface gravities from dynamical modeling and asteroseismology nearly agree, while surface gravities from stellar atmosphere modeling are higher ($\log g_1 = 3.21 \pm 0.45$, $\log g_2 = 3.33 \pm 0.37$). A similar discrepancy has been found between the asteroseismic and spectroscopic surface gravities of other giant stars, but the physical cause is unknown. \revise{Radii from stellar evolution models are consistent with a pair of nearly-coeval stars either on the red giant branch with an age of approximately $8.3 \times 10^8$ years, or coeval stars on the horizontal branch with an age of about $9.4 \times 10^8$ years. However, the period spacing of mixed oscillation modes clearly indicates that the main oscillator in KIC 9246715 is on the secondary red clump, and we conclude that KIC 9246715 is a pair of secondary red clump stars.}