  The Large Magellanic Cloud (LMC) is home to many HII regions, which may lead
to significant outflows. We examine the LMC's multiphase gas ($T\sim10^{4-5}$
K) in HI, SII, SiIV, and CIV using 110 stellar sight lines from the HST's
Ultraviolet Legacy Library of Young Stars as Essential Standards (ULLYSES)
program. We develop a continuum fitting algorithm based on the concept of
Gaussian Process regression and identify reliable LMC interstellar absorption
over $v_{\rm helio}=175-375$ km s$^{-1}$. Our analyses show disk-wide ionized
outflows in SiIV and CIV across the LMC with bulk velocities of $|v_{\rm out,
bulk}|\sim20-60$ km s$^{-1}$, which indicates that most of the outflowing mass
is gravitationally bound. The outflows' column densities correlate with the
LMC's star formation rate surface densities ($\Sigma_{\rm SFR}$), and the
outflows with higher $\Sigma_{\rm SFR}$ tend to be more ionized. Considering
outflows from both sides of the LMC as traced by CIV, we conservatively
estimate a total outflow rate of $\dot{M}_{\rm out}\gtrsim 0.03~M_\odot {\rm
yr}^{-1}$ and a mass loading factor of $\eta\gtrsim 0.15$. We compare the LMC's
outflows with those detected in starburst galaxies and simulation predictions,
and find a universal scaling relation of $|v_{\rm out, bulk}|\propto
\Sigma_{\rm SFR}^{0.23}$ over a wide range of star-forming conditions
($\Sigma_{\rm SFR}\sim10^{-4.5}-10^{2}~M_\odot {\rm yr}^{-1} {\rm kpc}^{-2}$).
Lastly, we find that the outflows are co-rotating with the LMC's young stellar
disk and the velocity field does not seem to be significantly impacted by
external forces; we thus speculate on the existence of a bow shock leading the
LMC, which may have shielded the outflows from ram pressure as the LMC orbits
the Milky Way.
