  The most powerful superflares reaching 10$^{39}$erg bolometric energy are
from giant stars. The mechanism behind flaring is supposed to be the magnetic
reconnection, which is closely related to magnetic activity including
starspots. However, it is poorly understood, how the underlying magnetic dynamo
works and how the flare activity is related to the stellar properties which
eventually control the dynamo action. We analyse the flaring activity of KIC
2852961, a late-type giant star, in order to understand how the flare
statistics are related to that of other stars with flares and superflares and
what the role of the observed stellar properties in generating flares is. We
search for flares in the full Kepler dataset of the star by an automated
technique together with visual inspection. We set a final list of 59 verified
flares during the observing term. We calculate flare energies for the sample
and perform a statistical analysis. The stellar properties of KIC 2852961 are
revised and a more consistent set of parameters are proposed. The cumulative
flare energy distribution can be characterized by a broken power-law, i.e. on
the log-log representation the distribution function is fitted by two linear
functions with different slopes, depending on the energy range fitted. We find
that the total flare energy integrated over a few rotation periods correlates
with the average amplitude of the rotational modulation due to starspots.
Flares and superflares seem to be the result of the same physical mechanism at
different energetic levels, also implying that late-type stars in the main
sequence and flaring giant stars have the same underlying physical process for
emitting flares. There might be a scaling effect behind generating flares and
superflares in the sense that the higher the magnetic activity the higher the
overall magnetic energy released by flares and/or superflares.
