  We report the discovery of a sub-Jupiter mass planet orbiting beyond the snow
line of an M-dwarf most likely in the Galactic disk as part of the joint
Spitzer and ground-based monitoring of microlensing planetary anomalies toward
the Galactic bulge. The microlensing parameters are strongly constrained by the
light curve modeling and in particular by the Spitzer-based measurement of the
microlens parallax, $\pi_\mathrm{E}$. However, in contrast to many planetary
microlensing events, there are no caustic crossings, so the angular Einstein
radius, $\theta_\mathrm{E}$ has only an upper limit based on the light curve
modeling alone. Additionally, the analysis leads us to identify 8 degenerate
configurations: the four-fold microlensing parallax degeneracy being doubled by
a degeneracy in the caustic structure present at the level of the ground-based
solutions. To pinpoint the physical parameters, and at the same time to break
the parallax degeneracy, we make use of a series of arguments: the $\chi^2$
hierarchy, the Rich argument, and a prior Galactic model. The preferred
configuration is for a host at $D_L=3.73_{-0.67}^{+0.66}~\mathrm{kpc}$ with
mass $M_\mathrm{L}=0.30_{-0.12}^{+0.15}~\mathrm{M_\odot}$, orbited by a
Saturn-like planet with
$M_\mathrm{planet}=0.43_{-0.17}^{+0.21}~\mathrm{M_\mathrm{Jup}}$ at projected
separation $a_\perp = 1.70_{-0.39}^{+0.38}~\mathrm{au}$, about 2.1 times beyond
the system snow line. Therefore, it adds to the growing population of
sub-Jupiter planets orbiting near or beyond the snow line of M-dwarfs
discovered by microlensing. Based on the rules of the real-time protocol for
the selection of events to be followed up with Spitzer, this planet will not
enter the sample for measuring the Galactic distribution of planets.
