  We present ISO observations of the S(0), S(1), S(2), and S(3) rotational
lines of molecular hydrogen from two molecular clouds near the Galactic Center
(GC). We have also measured continuum dust emission at infrared wavelengths
with ISO and the rotational radio lines J=1-0 of 13CO and C18O and J=2-1 of
C18O with the IRAM-30m telescope. Using the dust continuum spectra and the CO
lines we derive a total visual extinction of 15-20 magnitudes toward these GC
clouds. After correcting the H2 data for extinction, the gas temperatures are
\~250 K and the column densities of warm gas are ~2e21 cm-2. This is the first
direct measure of the H2 column densities of the warm component; with this, we
estimate an NH3 abundance in the warm gas of ~ 2e-7. The column density of warm
gas is, at least, a factor of 100 larger than the corresponding column
densities derived from the warm dust. The observed ortho-to-para ratio (OTPR)
is ~ 1, clearly below the local thermodynamical equilibrium (LTE) OTPR for gas
at 250 K of ~3. Low velocity shocks (~ 10 km/s) are the most likely explanation
for the column densities of warm gas and dust and the non-LTE H2 OTPR.
