  The information on Galactic assembly time is imprinted on the chemodynamics
of globular clusters. This makes them important probes that help us to
understand the formation and evolution of the Milky Way. Discerning between
in-situ and ex-situ origin of these objects is difficult when we study the
Galactic bulge, which is the most complex and mixed component of the Milky Way.
To investigate the early evolution of the Galactic bulge, we analysed the
globular cluster NGC 6355. We derived chemical abundances and kinematic and
dynamic properties by gathering information from high-resolution spectroscopy
with FLAMES-UVES, photometry with the Hubble Space Telescope, and Galactic
dynamic calculations applied to the globular cluster NGC 6355. We derive an age
of $13.2\pm1.1$ Gyr and a metallicity of [Fe/H]$=-1.39\pm0.08$ for NGC 6355,
with $\alpha$-enhancement of [$\alpha$/Fe]$=+0.37\pm0.11$. The abundance
pattern of the globular cluster is compatible with bulge field RR Lyrae stars
and in-situ well-studied globular clusters. The orbital parameters suggest that
the cluster is currently confined within the bulge volume when we consider a
heliocentric distance of $8.54\pm0.19$ kpc and an extinction coefficient of
$R_V = 2.84\pm0.02$. NGC 6355 is highly likely to come from the main bulge
progenitor. {Nevertheless, it still} has a low probability of being formed from
an accreted event because its age is uncertain and because of the combined
[Mg/Mn] [Al/Fe] abundance. Its relatively low metallicity with respect to old
and moderately metal-poor inner Galaxy clusters may suggest a low-metallicity
floor for globular clusters that formed in-situ in the early Galactic bulge.
