  We report on one of the brightest flux levels of the Seyfert 2 galaxy NGC
2992 ever observed in X-rays, on May 2019. The source has been monitored every
few days from March 26, 2019 to December 14, 2019 by Swift-XRT, and
simultaneous XMM-Newton (250 ks) and NuSTAR (120 ks) observations were
triggered on May 6, 2019. The high count rate of the source (its 2-10 keV flux
ranged between 0.7 and $1.0\times10^{-10}$ erg cm$^{-2}$ s$^{-1}$) allows us to
perform a time-resolved spectroscopy, probing spatial scales of tens of
gravitational radii from the central black hole. By constructing a map of the
excess emission over the primary continuum, we find several emission structures
in the 5.0-7.2 keV energy band. From fitting the 50 EPIC pn spectral slices of
$\sim$5 ks duration, we interpret them as a constant narrow iron K$\alpha$ line
and three variable components in the iron K complex. When a self-consistent
model accounting for the accretion disk emission is considered (KYNrline), two
of these features (in the 5.0-5.8 keV and 6.8-7.2 keV bands) can be ascribed to
a flaring region of the accretion disk located at ${r_{in}}\simeq15$-40
r$_{g\rm }$ from the black hole. The third one (6.5-6.8 keV) is likely produced
at much larger radii ($r_{in}>50$ r$_{g\rm }$). The inner radius and the
azimuthal extension retrieved from the coadded spectra of the flaring states
are ${ r_{in}}=15\pm3$ r$_{g\rm }$ and $\phi=165^{\circ}-330^{\circ}$,
suggesting that the emitting region responsible for the broad iron K component
is a relatively compact annular sector within the disk. Our findings support a
physical scenario in which the accretion disk in NGC 2992 becomes more active
at high accretion rates ($L_{\rm bol}/L_{\rm Edd}\geq4\%$).
