  We present results of a pulsar population synthesis study that incorporates a
number of recent developments and some significant improvements over our
previous study. We have included the results of the Parkes multi-beam pulsar
survey in our select group of nine radio surveys, doubling our sample of radio
pulsars. We adopted with some modifications the radio beam geometry of
Arzoumanian, Chernoff & Cordes (2002). For the $\gamma$-ray beam, we have
assumed the slot gap geometry described in the work of Muslimov & Harding
(2003). To account for the shape of the distribution of radio pulsars in the
$\dot P-P$ diagram, we continue to find that decay of the magnetic field on a
timescale of 2.8 Myr is needed. With all nine surveys, our model predicts that
EGRET should have seen 7 radio-quiet (below the sensitivity of these radio
surveys) and 19 radio-loud $\gamma$-ray pulsars. AGILE (nominal sensitivity
map) is expected to detect 13 radio-quiet and 37 radio-loud $\gamma$-ray
pulsars, while GLAST, with greater sensitivity is expected to detect 276
radio-quiet and 344 radio-loud $\gamma$-ray pulsars. When the Parkes multi-beam
pulsar survey is excluded, the ratio of radio-loud to radio-quiet $\gamma$-ray
pulsars decreases, especially for GLAST. The decrease for EGRET is 45%,
implying that some fraction of EGRET unidentified sources are radio-loud
$\gamma$-ray pulsars. In the radio geometry adopted, short period pulsars are
core dominated. Unlike the EGRET $\gamma$-ray pulsars, our model predicts that
when two $\gamma$-ray peaks appear in the pulse profile, a dominant radio core
peak appears in between the $\gamma$-ray peaks. Our findings suggest that
further improvements are required in describing both the radio and $\gamma$-ray
geometries.
