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To examine the observed properties of dwarf galaxies in the LG, we use the compilation from \citet{McConnachie2012}, which includes all galaxies known at that time within $3 \mpc$ of the Sun.  %We select ``dwarf'' galaxies as $\mstar\lesssim10^9\msun$, including the LMC ($\mstar=1.5\times10^9\msun$).  We also include the more recent measurements or upper limits of cold atomic gas mass from \citet{Spekkens2014}.  We %We  do not include the recently discovered ultra-faint satellites of the MW from the Dark Energy Survey \citep{Koposov2015, DES2015}, though if they are all quiescent, their inclusion would not change our results. We define ``satellite'' galaxies as those within $300\kpc$ of either the MW or M31, motivated by the observed sharp transition in star formation, gas, and morphological properties within this distance.  %$300\kpc$ also coincides with the median virial radius, $\rvir$, for our simulated MW/M31 halos (see below).