  We investigate the metallicity, age, and orbital anatomy of the inner Milky
Way, specifically focussing on the outer bar region. We integrated a sample of
APOGEE DR16 inner Galaxy stars in a state of the art bar-bulge potential with a
slow pattern speed and investigated the link between the resulting orbits and
their [Fe/H] and ages. By superimposing the orbits, we built density, [Fe/H],
and age maps of the inner Milky Way, which we divided further using the orbital
parameters eccentricity, |Xmax|, and |Zmax|. We find that at low heights from
the Galactic plane, the Galactic bar gradually transitions into a radially
thick, vertically thin, elongated inner ring with average solar [Fe/H]. This
inner ring is mainly composed of stars with AstroNN ages between 4 and 9 Gyr
with a peak in age between 6 and 8 Gyr, making the average age of the ring ~6
Gyr. The vertical thickness of the ring decreases markedly towards younger
ages. We also find very large L4 Lagrange orbits that have average solar to
super-solar metallicities and intermediate ages. Lastly, we confirm a clear
X-shape in the [Fe/H] and density distributions at large Galactic heights. The
orbital structure obtained for the APOGEE stars reveals that the Milky Way
hosts an inner ring-like structure between the planar bar and corotation. This
structure is on average metal rich, intermediately aged, and enhances the
horizontal metallicity gradient along the bar's major axis.
