  The Galactic Anticenter Stellar Structure (GASS) has been identified with
excess surface densities of field stars in several large area sky surveys, and
with an unusual, string-like grouping of five globular clusters. At least two
of these are diffuse, young ``transitional'' clusters between open and globular
types. Here we call attention to the fact that four {\it younger} open or
transitional clusters extend the previously identified, string-like cluster
grouping, with at least one having a radial velocity consistent with the
previously found GASS velocity-longitude trend. All nine clusters lie close to
a plane tipped 17$\arcdeg$ to the Galactic plane. This planar orientation is
used to forage for additional potential cluster members in the inner Galaxy,
and a number are found along the same plane and string-like sequence, {\it
including almost all fifteen known outer, old open clusters}. Tidal accretion
of a dwarf satellite galaxy on a low inclination orbit -- perhaps the GASS
system -- appears to be a plausible explanation for the origin of the outer,
old open and transitional clusters of the Milky Way. We use these clusters to
explore the age-metallicity relation of the putative accreted GASS progenitor.
Finally, we provide the first radial velocity of a star in the cluster BH 176
and discuss its implications.
