  The Laser Interferometer Space Antenna (LISA) is expected to detect a wide
variety of gravitational wave sources in the mHz band. Some of these signals
will elude individual detection, instead contributing as confusion noise to one
of several stochastic gravitational-wave backgrounds (SGWBs) -- notably
including the `Galactic foreground', a loud signal resulting from the
superposition of millions of unresolved double white dwarf binaries (DWDs) in
the Milky Way. It is possible that similar, weaker SGWBs will be detectable
from other DWD populations in the local universe, including the Large
Magellanic Cloud (LMC). We use the Bayesian LISA Inference Package
($\tt{BLIP}$) to investigate the possibility of an anisotropic SGWB generated
by unresolved DWDs in the LMC. To do so, we compute the LMC SGWB from a
realistic DWD population generated via binary population synthesis, simulate
four years of time-domain data with $\tt{BLIP}$ comprised of stochastic
contributions from the LMC SGWB and the LISA detector noise, and analyze this
data with $\tt{BLIP}$'s spherical harmonic anisotropic SGWB search. We also
consider the case of spectral separation from the Galactic foreground. We
present the results of these analyses and show, for the first time, that the
unresolved DWDs in the LMC will comprise a significant SGWB for LISA.
