  We analyze the OVI content and kinematics for 126 $z < 1$ HI-selected
absorbers for which the metallicities of their cool photoionized phase have
been determined. We separate the absorbers into 100 strong Lya forest systems
(SLFSs with $15 \lesssim$ logN(HI) $< 16.2$) and 26 partial Lyman Limit systems
(pLLSs with $16.2 \leq$ logN(HI) $\leq 17.2$). The sample is drawn from the COS
CGM Compendium (CCC) of Lehner et al. and has OVI coverage in $S/N \geq 8$
HST/COS G130M/G160M QSO spectra, yielding a $2\sigma$ completeness level of
logN(OVI) $\geq 13.6$. There are significant differences in the OVI detection
rates between low-metal (LM; [X/H] $\leq -1.4$) SLFSs and high-metal (HM; [X/H]
$> -1.4$) SLFSs, $\sim$15\% versus $\sim$60%, respectively. The OVI frequency
for the HM and LM pLLSs is, however, similar $\sim$60%. The SLFSs and pLLSs
with no OVI are consistent with gas being in a single-phase, while those with
OVI trace multiphase gas. We find that the OVI velocity widths and column
densities have different distributions in LM and HM gas. We observe a strong
correlation between OVI column density and metallicity. The strongest
(logN(OVI) $\gtrsim 14$) and broadest OVI absorbers are nearly systematically
found to be associated with HM gas, while weaker OVI absorbers are found in
both LM and HM HI-bearing gas. From comparisons with galaxy and OVI surveys, we
conclude absorbers with logN(OVI) $\gtrsim 14$ most likely arise in the
circumgalactic medium (CGM) of star-forming galaxies, with the broadest and
strongest possibly tracing galaxy outflows. Absorbers with weak OVI most likely
trace the extended CGM or intergalactic medium (IGM), while those without OVI
in all likelihood originate in the IGM.
