  We have investigated the molecular environment of the semicircular composite
supernova remnant (SNR) 3C396 and performed a Chandra spatially resolved
thermal X-ray spectroscopic study of this young SNR. With our CO millimeter
observations, we find that the molecular clouds (MCs) at V(LSR)~84km/s can
better explain the multiwavelength properties of the remnant than the
V(LSR)=67-72km/s MCs that are suggested by Lee et al. (2009). At around 84km/s,
the western boundary of the SNR is perfectly confined by the western molecular
wall. The CO emission fades out from west to east, indicating that the eastern
region is of low gas density. In particular, an intruding finger/pillar-like
MC, which may be shocked at the tip, can well explain the X-ray and radio
enhancement in the southwest and some infrared filaments there. The SNR-MC
interaction is also favored by the relatively elevated 12CO J=2-1/J=1-0 line
ratios in the southwestern "pillar tip" and the molecular patch on the
northwestern boundary. The redshifted 12CO (J=1-0 and J=2-1) wings (86-90km/s)
of an eastern 81km/s molecular patch may be the kinematic evidence for shock-MC
interaction. We suggest that the 69km/s MCs are in the foreground based on HI
self-absorption while the 84km/s MCs at a distance of 6.2 kpc (the tangent
point) are in physical contact with SNR 3C396. The X-ray spectral analysis
suggests an SNR age of ~3kyr. The metal enrichment of the X-ray emitting gas in
the north and south implies a 13-15Msun B1-B2 progenitor star.
