  We present a multi-zone galactic chemical evolution (GCE) model for the Milky
Way that takes the most recently updated yields of major nucleosynthesis
channels into account. It incorporates physical processes commonly found in
previous GCE models like supernova and star formation feedback, the radial flow
of gas in the disk, and the infall of fresh gas, along with stellar scattering
processes like radial migration. We individually analyse the effect of
different physical processes present in our model on the observed properties of
the Galaxy. The radial flow of gas in the disk plays an important role in
establishing the radial gradient for \feh{} in the low-\alphafe{} sequence. Our
model with one episode of smooth gas infall and constant star formation
efficiency is capable of reproducing the observed \fehalpha{} distribution of
stars at different ($R$, $|z|$) positions in the Milky Way. Our results point
to the rapid evolution of \alphafe{} after the onset of Type Ia supernovae and
a high star formation rate during the formation of the high-\alphafe{} sequence
as the origin of dual peaks in \alphafe{}. A secondary infall is unnecessary to
reproduce the \alphafe{}-gap and chemical spread in the disk in our model. We
additionally compare the median age for various mono-abundance populations and
the age-metallicity relation at different ($R$, $|z|$) positions from our
fiducial model to observations. We discuss our results in relation to other
related work in detail.
