  The inner $\sim5$ kiloparsec (kpc) region of the Milky Way is complex.
Unravelling the evolution of the Galaxy requires precise understanding of the
formation of this region. We report a study focused on disentangling the inner
Galaxy ($r < 5$ kpc) using the measured positions, velocities, and element
abundance ratios of red giant stars from the $APOGEE-Gaia$ surveys. After
removing the stellar halo, inner Galaxy populations can be grouped into three
main components based on their angular momentum: bar, disc, and a previously
unreported ``knot'' component. The knot has a spheroidal shape, is concentrated
in the inner $\sim1.5$ kpc, is comprised of stars on nearly-radial orbits, and
contains stars with super-solar [Fe/H] element abundances. The chemical
compositions of the knot are qualitatively similar to the Galactic bar and
inner disc, suggestive that these three populations share a common genesis; the
chemical/dynamic properties of the knot suggest it could constitute a classical
bulge formed via secular evolution. Moreover, our results show that the bar is
more slowly rotating than previously thought, with a pattern speed of
$\Omega_{\mathrm{bar}}=24\pm3$ km s$^{-1}$ kpc$^{-1}$. This new estimate
suggests that the influence of the bar extends beyond the solar radius, with
$R_{\mathrm{CR}}\sim9.4-9.8$ kpc, depending on the adopted Milky Way rotation
curve; it also suggests a ratio of corotation to bar length of
$\mathcal{R}\sim1.8-2$. Our findings help place constraints on the formation
and evolution of inner Galaxy populations, and directly constrain dynamical
studies of the Milky Way bar and stars in the solar neighbourhood.
