  We report preliminary results of large-scale distribution toward the
Magellanic supernova remnant N132D using Mopra and Chandra archival datasets.
We identified a cavity-like CO structure along the X-ray shell toward the
southern half of it. The total mass of associating molecular gas is $\sim10^4
M_\odot$, which is smaller than the previous study by an order of magnitude.
Further observations using ALMA, ASTE, and Mopra will reveal the detailed
spatial structures and its physical conditions.
