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tokens: field is obtained using the cloud-in-cells particle assignment scheme (CIC; e.g. Hockney Eastwood 1981 ). We introduce some scatter before the mapping procedure in a way that is different from the original EZmock paper. The new scattering formula is where and are the ZA density field after and before the scattering, respectively, and G (λ) is a random number drawn from the Gaussian distribution with width λ. The exponential function, exp[ G (λ)], is used to avoid negative densities. The term including ρ a introduces a non-linear mapping, which converges to 1 when is large. It plays a similar role as the density saturation parameter in the original EZmock paper. Furthermore, we apply a density cut ρ c (called the density threshold in Chuang et al. 2015a ) on the ZA density field before applying the scatter formula to make sure that there is no object produced in a low-density region. The mock catalogue is then populated by randomly picking a fraction of the original ZA particles in each cell, which is equal to the number of haloes attributed to it by the PDF mapping procedure described above. Finally, we assign the velocity by multiplying the displacement field by a factor f , and combining it with a three-dimensional Gaussian random motion with width σ . The factor f is computed by where f () and H () are the growth rate and Hubble parameter, respectively, at the redshift of the simulation box. Thus, we have five effective bias parameters ( n d , A , λ, ρ c and σ ) to adjust EZmocks. In contrast to Chuang et al. ( 2015a ), we do not modify the input power spectrum for calibration because we want to observe the impact of different cosmological models, as explained in the next section. 2.2 Simulation set-up We use the same input power spectrum as the one used by Chuang et al. ( 2015a ), that is ΛCDM Planck cosmology with {Ω M = 0.307115, Ω b = 0.048206, σ 8 = 0.8288, n s = 0.96}, and a Hubble constant () given by h = 0.6777. The output galaxy catalogues are at redshift = 0.5618. Again, following Chuang et al. ( 2015a ), we calibrate the number density to 3.5 × 10 −4 , which is similar to that of the SDSS-III/Baryon Oscillation Spectroscopic Survey (BOSS) galaxy sample at ∼ 0.5 (Reid et al. 2016 ). The simulation boxes are 2.5 h −1 Gpc each side. The particle mesh used is 960 3 . We construct three sets of 3000 EZmock simulation boxes with three sets of parameters. These three sets of boxes share the same 3000 Gaussian random fields. Table 1 lists the values of these parameters. The first set is the reference, whose clustering statistics are similar to those in Chuang et al. ( 2015a ) but not the same, because the EZmock methodology we are using here is slightly different, as mentioned above. Table 1. The three sets of EZmock parameters used in this study. We construct 3000 EZmock simulation boxes for each set of parameters (i.e. 9000 boxes in total). The second set of 3000 EZmocks has a different amplitude in the input power spectrum (i.e.