  Context. Understanding the conditions in which stars and stellar clusters
form is of great importance. In particular the role that stellar feedback may
have is still hampered by large uncertainties. Aims. We investigate the role
played by ionising radiation and protostellar outflows during the formation and
evolution of a stellar cluster. To self-consistently take into account gas
accretion, we start with clumps of tens of parsecs in size. Methods. Using an
adaptive mesh refinement code, we run magneto-hydrodynamical numerical
simulations aiming at describing the collapse of massive clumps with either no
stellar feedback or taking into account ionising radiation and/or protostellar
jets. Results. Stellar feedback substantially modifies the protostellar cluster
properties, in several ways. We confirm that protostellar outflows reduce the
star formation rate by a factor of a few, although the outflows do not stop
accretion and likely enough do not modify the final cluster mass. On the other
hand, ionising radiation, once sufficiently massive stars have formed,
efficiently expels the remaining gas and reduces the final cluster mass by a
factor of several. We found that while HII radiation and jets barely change the
distribution of high density gas, the latter increases, at a few places, the
dense gas velocity dispersion again by a factor of several. As we are starting
from a relatively large scale, we found that the clusters whose mass and size
are respectively on the order of a few 1000 M and a fraction of parsec, present
a significant level of rotation. Moreover we found that the sink particles
which mimic the stars themselves, tend to have rotation axis aligned with the
cluster large scale rotation. Finally, computing the classical Q parameter used
to quantify stellar cluster structure, we infer that when jets are included in
the calculation, [...]
