  We present a one-dimensional radiation-hydrodynamic model of a spherically
symmetric cloud evolving under the influence of the self-gravity and the
feedback from a star cluster forming in its centre. On one hand, the model is
simple due to its 1D geometry, on the other hand, the feedback includes the
ionising radiation, stellar winds and the radiation pressure acting on gas and
dust. The star cluster is formed from the gas flowing into the cloud centre and
the feedback parameters are determined from stellar evolution models and the
cluster star forming history. The model is compared to the semi-analytic code
WARPFIELD implementing similar physical processes and exploring the scenario
that the young cluster R136 in the Large Magellanic Cloud was formed due to
re-collapse of the shell formed by the previous generation star cluster. A good
qualitative agreement is found, however, $3 - 4$ times higher stellar mass is
needed to disrupt the cloud in our model, because it takes into account
(contrary to WARPFIELD) self-gravity of the cloud surrounding the shell. We use
the model to explore star formation in clouds with different mass, radius and
density profile measuring their star formation efficiency (SFE), i.e. the
fraction of the cloud mass converted to stars. We found that SFE is a function
of a single parameter, $\mathrm{log(SFE)} \propto -n_{hm}^{-0.46}$, with
$n_{hm}$ being the cloud mean particle density within its half-mass radius.
Furthermore, we found that the feedback efficiency, i.e. a fraction of the
feedback energy retained by gas, has a nearly constant value $\sim 10^{-3}$.
