  From integral field data we extract the optical spectra of 20 shocked clouds
in the supernova remnant N132D in the Large Magellanic Cloud (LMC). Using
self-consistent shock modelling, we derive the shock velocity, pre-shock cloud
density and shock ram pressure in these clouds. We show that the [Fe X] and [Fe
XIV] emission arises in faster, partially radiative shocks moving through the
lower density gas near the periphery of the clouds. In these shocks dust has
been effectively destroyed, while in the slower cloud shocks the dust
destruction is incomplete until the recombination zone of the shock has been
reached. These dense interstellar clouds provide a sampling of the general
interstellar medium (ISM) of the LMC. Our shock analysis allows us to make a
new determination of the ISM chemical composition in N, O, Ne, S, Cl and Ar,
and to obtain accurate estimates of the fraction of refractory grains
destroyed. From the derived cloud shock parameters, we estimate cloud masses
and show that the clouds previously existed as typical self-gravitating
Bonnor-Ebert spheres into which converging cloud shocks are now being driven.
