  We present a detailed chemical abundance study of seven giant stars in M68
including six red giants and one post-AGB star. We find significant differences
in the gravities determined using photometry and those obtained from ionization
balance, which suggests that non-LTE effects are important for these
low-gravity, metal-poor stars. We adopt an iron abundance using photometric
gravities and Fe II lines to minimize those effects, finding [Fe/H] = -2.16 +/-
0.02. For element-to-iron ratios,we rely on neutral lines vs. Fe I and ionized
lines vs. FeII (except for [O/Fe]) to also minimize non-LTE effects.
  We find variations in the abundances of sodium among the program stars.
However, there is no correlation (or anti-correlation) with the oxygen
abundances. Further, the post-AGB star has a normal (low) abundance of sodium.
Both of these facts add further support to the idea that the variations seen
among some light elements within individual globular clusters arises from
primordial variations, and not from deep mixing.
  M68, like M15, shows elevated abundances of silicon compared to other
globular clusters and comparable metallicity field stars. But M68 deviates even
more in showing a relative underabundance of titanium. We speculate that in
M68, titanium is behaving like an iron-peak element rather than its more
commonly observed adherence to enhancements seen in the "alpha" elements such
as magnesium, silicon, and calcium. We interpret this result as implying that
the chemical enrichment seen in M68 may have arisen from contributions from
supernovae with somewhat more massive progenitors than contribute normally to
abundances seen in other globular clusters.
