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In this paper, we examine AM transport due to convectively excited IGW within massive stars, focusing primarily on AM transport due to late burning stages (He, C, O, and Si burning). We find that IGW are generally capable of redistributing large amounts of AM before CC despite the short stellar evolution time scales. IGW emitted from convective shells propagate into the radiative core and can substantially slow its rotation. We also show that stochastic influxes of AM via IGW set a minimum core rotation rate which may account for a large population of slowly rotating ($P \gtrsim 100 \,{\rm ms}$) NSs.  Our paper is organized as follows. In Section 2, we describe our massive star models, the generation of IGW during various stages of stellar evolution, and the AM they transport. In Section 3, we ivestigatethe consequences of IGW AM transport and examine  whether the IGW can spin down the cores of massive stars, attempting to determine a minimum core  rotation period in the presence of IGW. We also period. In Section 4, we  consider whether IGW can stochastically spin up a very slowly rotating core, attempting to determine a maximum core  rotation period for the pre-collapse core. period.  In Section 4, 5,  we conclude with a discussion of our results and their implications for core collapse, supernovae, and the birth of compact objects.