  The Laser Interferometer Space Antenna (LISA) will unveil the non-transient
gravitational wave sky full of inspiralling stellar-mass compact binaries
within the Local Universe. The Large Magellanic Cloud (LMC) is expected to be
prominent on the LISA sky due to its proximity and its large population of
double white dwarfs (DWD). Here we present the first dedicated study of the LMC
with gravitational wave sources. We assemble three LMC models based on: (1) the
density distribution and star formation history from optical wavelength
observations, (2) a detailed hydrodynamic simulation, and (3) combining the
two. Our models yield a hundred to several hundred detectable DWDs: indeed, the
LMC will be a resolved galaxy in the LISA sky. Importantly, amongst these we
forecast a few tens to a hundred double degenerate supernovae type Ia
progenitors, a class of binaries which have never been unambiguously observed.
The range in the number of detections is primarily due to differences in the
LMC total stellar mass and recent star formation in our models. Our results
suggest that the total number, periods, and chirp masses of LISA sources may
provide independent constraints on both LMC stellar mass and recent star
formation by comparing LISA observations with the models, although such
constraints will be highly model-dependent. Our publicly available model
populations may be used in future studies of the LMC, including its structure
and contribution to LISA confusion noise.
