The paper develops an analytic model to understand the spatial distribution of dark matter haloes relative to the underlying mass distribution. The model is based on an extension of the Press-Schechter formalism to account for the statistical distribution of dark haloes within an initially Gaussian density field. Gravitationally induced motions are treated using a spherical collapse approximation. The model is tested against N-body simulations and found to accurately describe the bias function, which relates the mean overdensity of haloes of mass \(M\) within spheres of radius \(R\) and mass overdensity \(\delta\). This bias function is sufficient to calculate the cross-correlation between dark haloes and mass, showing excellent agreement with simulation results. The model also predicts the autocorrelation function of dark haloes, which is proportional to that of the mass over a wide range of scales. The results have implications for understanding galaxy biasing and reconstructing the cosmic mass distribution from observations.The paper develops an analytic model to understand the spatial distribution of dark matter haloes relative to the underlying mass distribution. The model is based on an extension of the Press-Schechter formalism to account for the statistical distribution of dark haloes within an initially Gaussian density field. Gravitationally induced motions are treated using a spherical collapse approximation. The model is tested against N-body simulations and found to accurately describe the bias function, which relates the mean overdensity of haloes of mass \(M\) within spheres of radius \(R\) and mass overdensity \(\delta\). This bias function is sufficient to calculate the cross-correlation between dark haloes and mass, showing excellent agreement with simulation results. The model also predicts the autocorrelation function of dark haloes, which is proportional to that of the mass over a wide range of scales. The results have implications for understanding galaxy biasing and reconstructing the cosmic mass distribution from observations.