  In this paper, we build from previous work (Bustard et al. 2018) and present
simulations of recent (within the past Gyr), magnetized, cosmic ray driven
outflows from the Large Magellanic Cloud (LMC), including our first attempts to
explicitly use the derived star formation history of the LMC to seed outflow
generation. We run a parameter set of simulations for different LMC gas masses
and cosmic ray transport treatments, and we make preliminary comparisons to
published outflow flux estimates, neutral and ionized hydrogen observations,
and Faraday rotation measure maps. We additionally report on the gas mass that
becomes unbound from the LMC disk and swept by ram pressure into the Trailing
Magellanic Stream. We find that, even for our largest outburst, the mass
contribution to the Stream is still quite small, as much of the
outflow-turned-halo gas is shielded on the LMC's far-side due to the LMC's
primarily face-on infall through the Milky Way halo over the past Gyr. On the
LMC's near-side, past outflows have fought an uphill battle against ram
pressure, with near-side halo mass being at least a factor of a few smaller
than the far-side. Absorption line studies probing only the LMC foreground,
then, may be severely underestimating the total mass of the LMC halo formed by
outflows.
