  We present independent and self-consistent metallicities for a sample of 807
planet-hosting stars from the California-Kepler Survey from an LTE
spectroscopic analysis using a selected sample of Fe I and Fe II lines.
Correlations between host-star metallicities, planet radii, and planetary
architecture (orbital periods - warm or hot - and multiplicity - single or
multiple), were investigated using non-parametric statistical tests. In
addition to confirming previous results from the literature, e.g., that overall
host star metallicity distributions differ between hot and warm planetary
systems of all types, we report on a new finding that when comparing the median
metallicities of hot versus warm systems, the difference for multiple
Super-Earths is considerably larger when compared to that difference in single
Super-Earths. The metallicity CDFs of hot single Super-Earths versus warm
single Super-Earths indicate different parent stellar populations, while for
Sub-Neptunes this is not the case. The transition radius between Sub-Neptunes
and Sub-Saturns was examined by comparing the APOGEE metallicity distribution
for the Milky Way thin disk in the solar neighborhood with metallicity
distributions of host stars segregated based upon the largest known planet in
their system. These comparisons reveal increasingly different metallicity
distributions as the radius of the largest planet in the systems increases,
with the parent stellar metallicities becoming significantly different for
R$_{p}>$ 2.7 R$_{\oplus}$. The behavior of the p-values as a function of planet
radius undergoes a large slope change at R$_{p}$ = 4.4 $\pm$ 0.5 R$_{\oplus}$,
indicating the radius boundary between small and large planets.
