  We explore the dynamics of a ``cluster wind'' flow in the regime in which the
shocks resulting from the interaction of winds from nearby stars are radiative.
We first show that for a cluster with T Tauri stars and/or Herbig Ae/Be stars,
the wind interactions are indeed likely to be radiative. We then compute a set
of four, three dimensional, radiative simulations of a cluster of 75 young
stars, exploring the effects of varying the wind parameters and the density of
the initial ISM that permeates the volume of the cluster. These simulations
show that the ISM is compressed by the action of the winds into a structure of
dense knots and filaments. The structures that are produced resemble in a
qualitative way the observations of the IRAS 18511+0146 of Vig et al. (2007).
