  We report on the analysis of a microlensing event OGLE-2014-BLG-1722 that
showed two distinct short term anomalies. The best fit model to the observed
light curves shows that the two anomalies are explained with two planetary mass
ratio companions to the primary lens. Although a binary source model is also
able to explain the second anomaly, it is marginally ruled out by 3.1 $\sigma$.
The 2-planet model indicates that the first anomaly was caused by planet "b"
with a mass ratio of $q = (4.5_{-0.6}^{+0.7}) \times 10^{-4}$ and projected
separation in unit of the Einstein radius, $s = 0.753 \pm 0.004$. The second
anomaly reveals planet "c" with a mass ratio of $q_{2} = (7.0_{-1.7}^{+2.3})
\times 10^{-4}$ with $\Delta \chi^{2} \sim 170$ compared to the single planet
model. Its separation has a so-called close-wide degeneracy. We estimated the
physical parameters of the lens system from Bayesian analysis. This gives that
the masses of planet b and c are $m_{\rm b} = 56_{-33}^{+51}\,M_{\oplus}$ and
$m_{\rm c} = 85_{-51}^{+86}\,M_{\oplus}$, respectively, and they orbit a late
type star with a mass of $M_{\rm host} = 0.40_{-0.24}^{+0.36}\,M_{\odot}$
located at $D_{\rm L} = 6.4_{-1.8}^{+1.3}\,\rm kpc$ from us. If the 2-planet
model is true, this is the third multiple planet system detected by using the
microlensing method, and the first multiple planet system detected in the low
magnification events, which are dominant in the microlensing survey data. The
occurrence rate of multiple cold gas giant systems is estimated using the two
such detections and a simple extrapolation of the survey sensitivity of 6 year
MOA microlensing survey (Suzuki et al. 2016) combined with the 4 year $\mu$FUN
detection efficiency (Gould et al. 2010). It is estimated that $6 \pm 2\,\%$ of
stars host two cold giant planets.
