  Recently much progress has been made in probing the embedded stages of
massive star formation, pointing to formation scenarios akin to a scaled up
version of low-mass star formation. However, the latest stages of massive star
formation have rarely been observed. Using 1st and 2nd overtone CO bandhead
emission and near- to mid-infrared photometry we aim to characterize the
remnant formation disks around 5 unique pre-main-sequence (PMS) stars with
masses $6-12~\rm M_{\odot}$, that have constrained stellar parameters thanks to
their detectable photospheres. We seek to understand this emission and the
disks it originates from in the context of the evolutionary stage of the
studied sources. We use an analytic LTE disk model to fit the CO bandhead and
the dust emission, found to originate in different disk regions. For the first
time we modeled the 2nd overtone emission. Furthermore, we fit continuum
normalized bandheads and show the importance of this in constraining the
emission region. We also include $^{13}\rm CO$ in our models as an additional
probe of the young nature of the studied objects. We find that the CO emission
originates in a narrow region close to the star (<1 AU) and under very similar
disk conditions (temperatures and densities) for the different objects. This is
consistent with previous modeling of this emission in a diverse range of young
stellar objects. We discuss these results in the context of the positions of
these PMS stars in the Hertzsprung-Russel diagram and the CO emission's
association with early age and high accretion rates in (massive) young stellar
objects. We conclude that, considering their mass range and for the fact that
their photospheres are detected, the M17 PMS stars are observed in a relatively
early formation stage. They are therefore excellent candidates for longer
wavelength studies to further constrain the end stages of massive star
formation.
