  Sagittarius A* exhibits frequent flaring activity across the electromagnetic
spectrum. Signatures of an orbiting hot spot have been identified in the
polarized millimeter wavelength light curves observed with ALMA in 2017
immediately after an X-ray flare. The nature of these hot spots remains
uncertain. We expanded existing theoretical hot-spot models created to describe
the Sgr A* polarized emission at millimeter wavelengths. We sampled the
posterior space, identifying best-fitting parameters and characterizing
uncertainties. Using the numerical radiative transfer code ipole, we defined a
semi-analytical model describing a ball of plasma orbiting Sgr A*, threaded
with a magnetic field and emitting synchrotron radiation. We then explored the
posterior space in the Bayesian framework of dynesty. We fit the static
background emission separately, using a radiatively inefficient accretion flow
model. We considered eight models with a varying level of complexity,
distinguished by choices regarding dynamically important cooling, non-Keplerian
motion, and magnetic field polarity. All models converge to realizations that
fit the data, but one model without cooling, non-Keplerian motion, and magnetic
field pointing toward us improved the fit significantly and also matched the
observed circular polarization. Our models represent observational data well
and allow testing various effects in a systematic manner. From our analysis, we
have inferred an inclination of $155-160$ deg, which corroborates previous
estimates, a preferred period of 90 minutes, and an orbital radius of $9-12$
gravitational radii. Our non-Keplerian models indicate a preference for an
orbital velocity of $0.6-0.9$ times the Keplerian value. Last, all our models
agree on a high dimensionless spin value ($a_{*}>0.8$), but the impact of spin
on the corresponding light curves is subdominant with respect to other
parameters.
