  In the long-term multi-frequency monitoring program of the microquasars with
RATAN-600 we discovered the giant flare from the X-ray binary Cygnus X-3 on 13
September 2016. It happened after 2000 days of the 'quiescent state' of the
source passed after the former giant flare (~18 Jy) in March 2011. We have
found that during this quiet period the hard X-ray flux (Swift/BAT, 15-50 keV)
and radio flux (RATAN-600, 11 GHz) have been strongly anti-correlated. Both
radio flares occurred after transitions of the microquasar to a 'hypersoft'
X-ray state that occurred in February 2011 and in the end of August 2016. The
giant flare was predicted by us in the first ATel #9416. Indeed after dramatic
decrease of the hard X-ray Swift 15-50 keV flux and RATAN 4-11 GHz fluxes (a
'quenched state') a small flare (0.7 Jy at 4-11 GHz) developed on MJD 57632 and
then on MJD 57644.5 almost simultaneously with X-rays radio flux rose from 0.01
to 15 Jy at 4.6 GHz during few days. The rise of the flaring flux is well
fitted by a exponential law that could be a initial phase of the relativistic
electrons generation by internal shock waves in the jets. Initially spectra
were optically thick at frequencies lower 2 GHz and optically thin at
frequencies higher 8 GHz with typical spectral index about -0.5. After maximum
of the flare radio fluxes at all frequencies faded out with the exponential law
(~ exp(-(t-t0)/2d) for 21.7 GHz).
