  We present ASCA observations of supernova remnant (SNR) G349.7+0.2. The
remnant has an irregular shell morphology and is interacting with a molecular
cloud, evident from the presence of OH(1720 MHz) masers and shocked molecular
gas. The X-ray morphology is consistent with that at radio wavelengths, with a
distinct enhancement in the south. The X-ray emission from the SNR is well
described by a model of a thermal plasma which has yet to reach ionization
equilibrium. The hydrogen column of ~6.0 X 10^{22} cm^{-2} is consistent with
the large distance to the remnant of ~22 kpc estimated from the maser
velocities. We derive an X-ray luminosity of L_x(0.5-10.0 keV)= 1.8 X 10^{37}
d_{22}^2 erg/s, which makes G349.7+0.2 one of the most X-ray luminous
shell-type SNRs known in the Galaxy. The age of the remnant is estimated to be
about 2800 yrs. The ambient density and pressure conditions appear similar to
those inferred for luminous compact SNRs found in starburst regions of other
galaxies, and provides support for the notion that these may be the result of
SNR evolution in the vicinity of dense molecular clouds.
