  The Galactic center (GC) provides a unique laboratory for a detailed
examination of the interplay between massive star formation and the nuclear
environment of our Galaxy. Here, we present an 100 ks Chandra ACIS observation
of the Arches and Quintuplet star clusters. We also report on a complementary
mapping of the dense molecular gas near the Arches cluster made with the Owens
Valley Millimeter Array. The number-flux relation of point-like X-ray sources
indicates an over-population of relatively bright X-ray sources, which are
apparently associated with the clusters. The sources in the core of the Arches
and Quintuplet clusters are most likely extreme colliding wind massive star
binaries. The diffuse X-ray emission from the core of the Arches cluster has a
spectrum showing a 6.7-keV emission line and a surface intensity profile
declining steeply with radius, indicating an origin in a cluster wind. In the
outer regions near the Arches cluster, the overall diffuse X-ray enhancement
demonstrates a bow shock morphology and is prominent in the Fe Kalpha 6.4-keV
line emission. Much of this enhancement may result from an ongoing collision
between the cluster and the adjacent molecular cloud. The older and less
compact Quintuplet cluster contains much weaker X-ray sources and diffuse
emission, probably originating from low-mass stellar objects as well as a
cluster wind. However, the overall population of these objects, constrained by
the observed total diffuse X-ray luminosities, is substantially smaller than
expected for both clusters. This deficiency of low-mass objects may be a
manifestation of the unique star formation environment of the Galactic center.
