  We present results of N-body simulations aimed at understanding the dynamics
of young stars near the Galactic center. Specifically, we model the inspiral of
a cluster core containing an intermediate mass black hole and $N \sim 50$
cluster stars in the gravitational potential of a supermassive black hole. We
first study the elliptic three-body problem to isolate issues of tidal
stripping and subsequent scattering, followed by full N-body simulations to
treat the internal dynamics consistently. We find that our simulations
reproduce several dynamical features of the observed population. These include
the observed inner edge of the claimed clockwise disk, as well as the thickness
of said disk. We find that high density clumps, such as that claimed for
IRS13E, also result generically from our simulations. However, not all features
of the observations are reproduced. In particular, the surface density profile
of the simulated disk scales as $\Sigma \propto r^{-0.75}$, which is
considerably shallower than that observed. Further, at no point is any
significant counter-rotating population formed.
