We present results of our Monte Carlo simulations of dense star clusters near the Galactic center.
These clusters sink toward the center of the Galaxy by dynamical friction. During their inspiral,
they may undergo core collapse and form an intermediate mass black hole by runaway collisions.
Such a cluster can reach within a parsec of the Galactic center where it disrupts and leaves many
young stars as well as a massive black hole in the region. This scenario provides a natural
explanation for the presence of the young stars observed near the Galactic center. We determine
the initial conditions for this scenario to work. In addition, we present the mass distribution
of the cluster stars with respect to the distance from the Galactic center.