  We report observations with the MIPS instrument aboard the {\it Spitzer Space
Telescope} (SST) of four supernova remnants (SNRs) believed to be the result of
core-collapse SNe: N132D (0525-69.6), N49B (0525-66.0), N23 (0506-68.0), and
0453-68.5. All four of these SNRs were detected in whole at 24 $\mu$m and in
part at 70 $\mu$m. Comparisons with {\it Chandra} broadband X-ray images show
an association of infrared (IR) emission with the blast wave. We attribute the
observed IR emission to dust that has been collisionally heated by electrons
and ions in the hot, X-ray emitting plasma, with grain size distributions
appropriate for the LMC and the destruction of small grains via sputtering by
ions. As with our earlier analysis of Type Ia SNRs, models can reproduce
observed 70/24 $\mu$m ratios only if effects from sputtering are included,
destroying small grains. We calculate the mass of dust swept up by the blast
wave in these remnants, and we derive a dust-to-gas mass ratio of several times
less than the often assumed value of 0.25% for the LMC. We believe that one
explanation for this discrepancy could be porous (fluffy) dust grains.
