  We present an extinction analysis of 9 paths through the LMC and SMC based on
FUSE observations. To date, just two LMC sight lines have probed dust grain
composition and size distributions in the Clouds using spectra including
wavelengths as short as 950 A. We supplement these with results from 4 regions
distinguished by their IR through UV extinction curves and grouped as LMCAvg,
LMC2, SMC bar and SMC wing. Despite the distinct characters of Milky Way and
Magellanic Cloud extinction, our results are generally analogous to those found
for Galactic curves in that the FUSE portions of each extinction curve are
described reasonably well by FM curves fitted only to longer wavelength data
and lack any dramatic new extinction features, and any deviations from the CCM
formalism continue into FUV wavelengths. An MEM analysis of these curves
suggests that LMCAvg and SMC wing sight lines require more silicon and/or
carbon in dust than current abundance measurements would allow, while the
requirements for LMC2 and SMC bar sight lines do not fully tax the available
reservoirs. An intermediate product of this analysis is the measurement of new
H_2 abundances in the Magellanic Clouds. Collectively considering Cloud sight
lines that possess significant H_2 column densities, E(B-V)/N(HI) ratios are
reduced by significant factors relative to the Galactic mean, whereas the
corresponding E(B-V)/N(H_2) values more closely resemble their Galactic
counterpart. These trends reflect the fact that among these sight lines
f(H_2)-values are lower than those common in the Milky Way for paths with
similar degrees of reddening.
