  The Milky Way's progenitor experienced several merger events which left their
imprints on the stellar halo, including the Gaia-Sausage/Enceladus. Recently,
it has been proposed that this event perturbed the proto-disk and gave rise to
a metal rich ([Fe/H] $>-1$) low angular momentum ($v_{\phi} < 100$ km/s)
stellar population. These stars have dynamical and chemical properties
different from the accreted stellar halo, but are continuous with the canonical
thick disk. In this letter, we use a hydrodynamical simulation of an isolated
galaxy which develops clumps that produce a bimodal thin$+$thick disk chemistry
to explore whether it forms such a population. We demonstrate clump scattering
forms a metal-rich, low angular momentum population, without the need for a
major merger. We show that, in the simulation, these stars have chemistry,
kinematics and density distribution in good agreement with those in the Milky
Way.
