  The computation of theoretical pulsar populations has been a major component
of pulsar studies since the 1970s. However, the majority of pulsar population
synthesis has only regarded isolated pulsar evolution. Those that have examined
pulsar evolution within binary systems tend to either treat binary evolution
poorly or evolve the pulsar population in an ad-hoc manner. Thus no complete
and direct comparison with observations of the pulsar population within the
Galactic disk has been possible to date. Described here is the first component
of what will be a complete synthetic pulsar population survey code. This
component is used to evolve both isolated and binary pulsars. Synthetic
observational surveys can then be performed on this population for a variety of
radio telescopes. The final tool used for completing this work will be a code
comprised of three components: stellar/binary evolution, Galactic kinematics
and survey selection effects. Results provided here support the need for
further (apparent) pulsar magnetic field decay during accretion, while they
conversely suggest the need for a re-evaluation of the assumed \textit{typical}
MSP formation process. Results also focus on reproducing the observed
$P\dot{P}$ diagram for Galactic pulsars and how this precludes short timescales
for standard pulsar exponential magnetic field decay. Finally, comparisons of
bulk pulsar population characteristics are made to observations displaying the
predictive power of this code, while we also show that under standard binary
evolutionary assumption binary pulsars may accrete much mass.
