  Context: Subdwarf B stars (sdBs) play a crucial role in stellar evolution,
asteroseismology, and far-UV radiation of early-type galaxies, and have been
intensively studied with observation and theory. It has theoretically been
predicted that sdBs with neutron star (NS) companions exist in the Galaxy, but
none have been discovered yet. This remains a puzzle in this field. In a
previous study (hereafter Paper I), we have studied the formation channels of
sdB+NS binaries from main-sequence (MS) stars plus NS binaries by establishing
a model grid, but it is still unclear how these binaries consisting of MS stars
and NS binaries came to be in the first place. Aims: We systematically study
the formation of sdB+NS binaries from their original zero-age main-sequence
progenitors. We bridge the gap left by our previous study in this way. We
obtain the statistical population properties of sdB+NS binaries and provide
some guidance for observational efforts. Methods: We first used Hurley's rapid
binary evolution code BSE to evolve 10^7 primordial binaries to the point where
the companions of NS+MS, NS+Hertzsprung gap (HG) star, and NS+Giant Branch (GB)
star binaries have just filled their Roche lobes. Next, we injected these
binaries into the model grid we developed in Paper I to obtain the properties
of the sdB+NS populations. We adopted two prescriptions of NS natal kicks.
Different values of common-envelope ejection efficiency were chosen to examine
the effect of common-envelope evolution on the results. Conclusions: Most
sdB+NS binaries are located in the Galactic disk with small RV semi-amplitudes.
SdB+NS binaries with large RV semi-amplitudes are expected to be strong GWR
sources, some of which could be detected by LISA in the future.
