  The outer Galaxy beyond the Outer Arm represents a promising opportunity to
study star formation in an environment vastly different from the solar
neighborhood. In our previous study, we identified 788 candidate star-forming
regions in the outer Galaxy (at galactocentric radii $R_{\rm G}$ $\ge$ 13.5
kpc) based on Wide-field Infrared Survey Explorer (WISE) mid-infrared (MIR)
all-sky survey. In this paper, we investigate the statistical properties of the
candidates and their parental molecular clouds derived from the Five College
Radio Astronomy Observatory (FCRAO) CO survey. We show that the molecular
clouds with candidates have a shallower slope of cloud mass function, a larger
fraction of clouds bound by self-gravity, and a larger density than the
molecular clouds without candidates. To investigate the star formation
efficiency (SFE) at different $R_{\rm G}$, we used two parameters: 1) the
fraction of molecular clouds with candidates and 2) the monochromatic MIR
luminosities of candidates per parental molecular cloud mass. We did not find
any clear correlation between SFE parameters and $R_{\rm G}$ at $R_{\rm G}$ of
13.5 kpc to 20.0 kpc, suggesting that the SFE is independent of environmental
parameters such as metallicity and gas surface density, which vary considerably
with $R_{\rm G}$. Previous studies reported that the SFE per year (SFE/yr)
derived from the star-formation rate surface density per total gas surface
density, HI plus H$_2$, decreases with increased $R_{\rm G}$. Our results might
suggest that the decreasing trend is due to a decrease in HI gas conversion to
H$_2$ gas.
