  We present a new method for tracing the evolution of BCGs from $z\sim 2$ to
$z\sim 0$. We conclude on the basis of semi-analytical models that the best
method to select BCG progenitors at $z\sim 2$ is a hybrid environmental density
and stellar mass ranking approach. Ultimately we are able to retrieve 45\% of
BCG progenitors. We apply this method on the CANDELS UDS data to construct a
progenitor sample at high redshift. We furthermore populate the comparisons in
local universe by using SDSS data with statistically likely contamination to
ensure a fair comparison between high and low redshifts. Using these samples we
demonstrate that the BCG sizes have grown by a factor of $\sim 3.2$ since
$z\sim 2$, and BCG progenitors are mainly late-type galaxies, exhibiting less
concentrated profiles than their early-type local counterparts. We find that
BCG progenitors have more disturbed morphologies. In contrast, local BCGs have
much smoother profiles. Moreover, we find that the stellar masses of BCGs have
grown by a factor of $\sim 2.5$ since $z\sim 2$, and the SFR of BCG progenitors
has a median value of 13.5 $M_\odot$yr$^{-1}$, much higher than their quiescent
local descendants. We demonstrate that over $z=1-2$ star formation and merging
contribute equally to BCG mass growth. However, merging plays a dominant role
in BCG assembly at $z \lesssim 1$. We also find that BCG progenitors at
high-$z$ are not significantly different from other galaxies of similar mass at
the same epoch. This suggests that the processes which differentiate BCGs from
normal massive elliptical galaxies must occur at $z \lesssim 2$.
