  We present a statistical analysis of the associated, high ionization narrow
absorption line (NAL) systems in a sample of 59 QSOs defined from the HST QSO
Absorption Line Key Project. We have compiled the QSO luminosities at 2500 A, 5
GHz, and 2 keV, spectral indices at 2500 A and 5 GHz, the H-beta emission line
FWHM, the CIV emission line FWHM, and the radio core fraction. We find 17
associated NALs toward 15 QSOs, of which ~10 are statistically expected to be
intrinsic. From a multivariate clustering analysis, the QSOs seem to group
together based primarily on radio luminosity, followed by radio spectral index,
CIV emission line FWHM, and soft X-ray luminosity. Radio-loud QSOs which have
compact radio morphologies, flat radio spectra, and mediocre CIV FWHM (<6000
km/s) do not have detectable associated NALs, down to REW(CIV)=0.35 A. We find
that BALQSOs have an enhanced probability of hosting detectable NAL gas and
that the velocities of associated NALs are peaked around the emission
redshifts, rather than the systemic redshifts of the QSOs. There is only one
strong NAL [REW(CIV)>1.5 A] in our low redshift sample which implies evolution
in the number of strong NALs with redshift. We interpret these results in the
context of an accretion-disk model. In this framework, we suggest that the
observational clues result from differences in orientation and wind properties,
the latter presumably associated with the QSO radio properties. (abridged)
