  (Abridged) The inner couple hundred pcs of our Galaxy is characterized by
significant amount of synchrotron-emitting gas, which appears to co-exist with
a large reservoir of molecular gas. The spatial correlation between fluorescent
Fe K-alpha line emission at 6.4 keV and molecular line emission from Galactic
center molecular clouds has been explained as reflected X-rays from a past
outburst of Sgr A*. Here we present multi-wavelength study of a representative
Galactic center cloud Sgr C using Chandra, VLA and FCRAO. We note a correlation
between the nonthermal radio filaments in Sgr C and the X-ray features,
suggesting that the two are related. We account for this distribution in terms
of the impact of the relativistic particles from local (nonthermal filaments)
and extended sources with diffuse neutral gas producing both a nonthermal
bremsstrahlung X-ray continuum emission, as well as diffuse 6.4 keV line
emission. The production rate of Fe Kalpha photons associated with the
injection of electrons into a cloud as a function of column density is
calculated. The required energy density of low-energy cosmic rays associated
with the synchrotron emitting radio filaments or extended features is estimated
to be in the range between 20 and $\sim10^3$ eV cm^-3 for Sgr C, Sgr B1, Sgr
B2, and ``the 45 and -30 \kms'' clouds. We also generalize this idea to explain
the pervasive production of diffuse Kalpha line and TeV emission from the
Galactic center molecular clouds. In particular, we suggest that IC scattering
of the sub-millimeter radiation from dust by relativistic electrons may
contribute substantially to the large-scale diffuse TeV emission observed
towards the central regions of the Galaxy.
