The initial mass function of stars - the number of stars N formed per interval of mass M - has long been known to be a power law, with d log N/d log M = ? = -1.3. Many explanations of this distribution have been advanced over the years, including fractal dimensions of star-forming molecular clouds and/or self-similar grouping of clouds. I will discuss simplified numerical simulations of star formation which show that gravitational accretion onto initial seed masses generates a power law mass distribution approaching ? ? -1 asymptotically, irrespective of complications of cloud structure. This mechanism can also explain the mass function of young star clusters, which also has a power law distribution with ? = -1. Finally, I will describe preliminary results concerning the origin of protostellar cloud angular momenta, including magnetic fields, with implications for the properties of protoplanetary disks that result from cloud collapse.