  In the $\Lambda$-Cold Dark Matter model of the Universe, galaxies form in
part through accreting satellite systems. Previous work have built an
understanding of the signatures of these processes contained within galactic
stellar halos. This work revisits that picture using seven Milky Way-like
galaxies in the \textit{Latte} suite of FIRE-2 cosmological simulations. The
resolution of these simulations allows a comparison of contributions from
satellites above M$_{*}$$\gtrsim$10$\times$$^{7}$M$_{\odot}$, enabling the
analysis of observable properties for disrupted satellites in a fully
self-consistent and cosmological context. Our results show that, the time of
accretion and the stellar mass of an accreted satellite are fundamental
parameters that in partnership dictate the resulting spatial distribution,
orbital energy, and [$\alpha$/Fe]-[Fe/H] compositions of the stellar debris of
such mergers $at$ $present$ $day$. These parameters also govern the resulting
dynamical state of an accreted galaxy at $z=0$, leading to the expectation that
the inner regions of the stellar halo (R$_{\mathrm{GC}}$ $\lesssim$30 kpc)
should contain fully phase-mixed debris from both lower and higher mass
satellites. In addition, we find that a significant fraction of the lower mass
satellites accreted at early times deposit debris in the outer halo
(R$_{\mathrm{GC}}$ $>$50 kpc) that are $not$ fully phased-mixed, indicating
that they could be identified in kinematic surveys. Our results suggest that,
as future surveys become increasingly able to map the outer halo of our Galaxy,
they may reveal the remnants of long-dead dwarf galaxies whose counterparts are
too faint to be seen $in$ $situ$ in higher redshift surveys.
