  Within a half-parsec from the Galactic center (GC), there is a population of
coeval young stars which appear to reside in a coherent disk. Surrounding this
dynamically-cool stellar system, there is a population of stars with a similar
age and much larger eccentricities and inclinations relative to the disk. We
propose a hypothesis for the origin of this dynamical dichotomy. Without
specifying any specific mechanism, we consider the possibility that both
stellar populations were formed within a disk some 6 Myr ago. But this orderly
structure was dynamically perturbed outside-in by an intruding object with a
mass ~10^4 Msun, which may be an intermediate-mass black hole (IMBH) or a dark
stellar cluster hosting an IMBH. We suggest that the perturber migrated inward
to ~0.15-0.3pc from the GC under the action of dynamical friction. Along the
way, it captured many stars in the outer disk region into its mean-motion
resonance, forced them to migrate with it, closely encountered with them, and
induced the growth of their eccentricity and inclination. But stars in the
inner regions of the disk retain their initial coplanar structure. We predict
that some of the inclined and eccentric stars surrounding the disk may have
similar Galactocentric semimajor axis. Future precision determination of their
kinematic distribution of these stars will not only provide a test for this
hypothesis but also evidences for the presence of an IMBH or a dark cluster at
the immediate proximity of the massive black hole at the GC. (abridged)
