  We use an extremely large volume ($2.4h^{-3}{\rm Gpc}^{3}$), high resolution
N-body simulation to measure the higher order clustering of dark matter haloes
as a function of mass and internal structure. As a result of the large
simulation volume and the use of a novel ``cross-moment'' counts-in-cells
technique which suppresses discreteness noise, we are able to measure the
clustering of haloes corresponding to rarer peaks than was possible in previous
studies; the rarest haloes for which we measure the variance are 100 times more
clustered than the dark matter. We are able to extract, for the first time,
halo bias parameters from linear up to fourth order. For all orders measured,
we find that the bias parameters are a strong function of mass for haloes more
massive than the characteristic mass $M_{*}$. Currently, no theoretical model
is able to reproduce this mass dependence closely. We find that the bias
parameters also depend on the internal structure of the halo up to fourth
order. For haloes more massive than $M_{*}$, we find that the more concentrated
haloes are more weakly clustered than the less concentrated ones. We see no
dependence of clustering on concentration for haloes with masses $M<M_{*}$;
this is contrary to the trend reported in the literature when segregating
haloes by their formation time. Our results are insensitive to whether haloes
are labelled by the total mass returned by the friends-of-friends group finder
or by the mass of the most massive substructure. This implies that our
conclusions are not an artefact of the particular choice of group finding
algorithm. Our results will provide important input to theoretical models of
galaxy clustering.
