  The object G2 was recently discovered descending into the gravitational
potential of the supermassive black hole (BH) Sgr A*. We test the photoionized
cloud scenario, determine the cloud properties, and estimate the emission
during the pericenter passage. The incident radiation is computed starting from
the individual stars at the locations of G2. The radiative transfer
calculations are conducted with CLOUDY code and $2011$ broadband and line
luminosities are fitted. The spherically symmetric, tidally distorted, and
magnetically arrested cloud shapes are tested with both the interstellar medium
dust and $10$~nm graphite dust. The best-fitting magnetically arrested model
has the initial density $n_{\rm init}=1.8\times10^5{\rm cm}^{-3}$, initial
radius $R_{\rm init}=2.2\times10^{15}{\rm cm}=17 {\rm mas}$, mass $m_{\rm
cloud}=4M_{\rm Earth}$, and dust relative abundance $A=0.072$. It provides a
good fit to $2011$ data, is consistent with the luminosities in $2004$ and
$2008$, and reaches an agreement with the observed size. We revise down the
predicted radio and X-ray bow shock luminosities to be below the quiescent
level of Sgr A*, which readily leads to non-detection in agreement to
observations. The magnetic energy dissipation in the cloud at the pericenter
coupled with more powerful irradiation may lead to an infrared source with an
apparent magnitude $m_{L'}\approx13.0$. No shock into the cloud and no X-rays
are expected from cloud squeezing by the ambient gas pressure. Larger than
previously estimated cloud mass $m_{\rm cloud}=(4-20)M_{\rm Earth}$ may produce
a higher accretion rate and a brighter state of Sgr A* as the debris descend
onto the BH.
