  Detailed chemical abundances of two stars in the intermediate-age Large
Magellanic Cloud (LMC) globular cluster NGC~1718 are presented, based on high
resolution spectroscopic observations with the MIKE spectrograph. The detailed
abundances confirm NGC~1718 to be a fairly metal-rich cluster, with an average
[Fe/H] ~ -0.55+/-0.01. The two red giants appear to have primordial O, Na, Mg,
and Al abundances, with no convincing signs of a composition difference between
the two stars---hence, based on these two stars, NGC~1718 shows no evidence for
hosting multiple populations. The Mg abundance is lower than Milky Way field
stars, but is similar to LMC field stars at the same metallicity. The previous
claims of very low [Mg/Fe] in NGC~1718 are therefore not supported in this
study. Other abundances (Si, Ca, Ti, V, Mn, Ni, Cu, Rb, Y, Zr, La, and Eu) all
follow the LMC field star trend, demonstrating yet again that (for most
elements) globular clusters trace the abundances of their host galaxy's field
stars. Similar to the field stars, NGC~1718 is found to be mildly deficient in
explosive $\alpha$-elements, but moderately to strongly deficient in O, Na, Mg,
Al, and Cu, elements which form during hydrostatic burning in massive stars.
NGC~1718 is also enhanced in La, suggesting that it was enriched in ejecta from
metal-poor AGB stars.
