  We have observed ten red giant stars in four old Large Magellanic Cloud
globular clusters with the high-resolution spectrograph MIKE on the Magellan
Landon Clay 6.5-m telescope. The stars in our sample have up to 20 elemental
abundance determinations for the alpha-, iron-peak, and neutron-capture element
groups. We have also derived abundances for the light odd-Z elements Na and Al.
We find NGC 2005 and NGC 2019 to be more metal-rich than previous estimates
from the Ca II triplet, and we derive [Fe/H] values closer to those obtained
from the slope of the red giant branch. However, we confirm previous
determinations for Hodge 11 and NGC 1898 to within 0.2 dex. The LMC cluster
[Mg/Fe] and [Si/Fe] ratios are comparable to the values observed in old
Galactic globular cluster stars, as are the abundances [Y/Fe], [Ba/Fe], and
[Eu/Fe]. The LMC clusters do not share the low-Y behavior observed in some
dwarf spheroidal galaxies. [Ca/Fe], [Ti/Fe], and [V/Fe] in the LMC, however,
are significantly lower than what is seen in the Galactic globular cluster
system. Neither does the behavior of [Cu/Fe] as a function of [Fe/H] in our LMC
clusters match the trend seen in the Galaxy, staying instead at a constant
value of ~0.8. Because not all [alpha/Fe] ratios are suppressed, these
abundance ratios cannot be attributed solely to the injection of Type Ia SNe
material, and instead reflect the differences in star formation history of the
LMC vs. the Milky Way. We conclude that many of the abundances in the LMC
globular clusters we observed are distinct from those observed in the Milky
Way, and these differences are intrinsic to the stars in those systems.
