We present the complete solution to a 95 \% scalar field cosmological model in which the dark matter is modeled by a scalar field \Phi with the scalar potential V ( \Phi ) = V _ { o } \left [ \cosh { ( \lambda \sqrt { \kappa _ { o } } \Phi ) } -1 \right ] and the dark energy is modeled by a scalar field \Psi , endowed with the scalar potential \tilde { V } ( \Psi ) = \tilde { V _ { o } } \left [ \sinh { ( \alpha \sqrt { \kappa _ { o } } \Psi ) } % \right ] ^ { \beta } .
This model has only two free parameters , \lambda and the equation of state \omega _ { \Psi } .
With these potentials , the fine tuning and the cosmic coincidence problems are ameliorated for both dark matter and dark energy and the models agrees with astronomical observations .
For the scalar dark matter , we clarify the meaning of a scalar Jeans lenght and then the model predicts a suppression of the Mass Power Spectrum for small scales having a wave number k > k _ { min, \Phi } , where k _ { min, \Phi } \simeq 4.5 h { Mpc } ^ { -1 } for \lambda \simeq 20.28 .
This last fact could help to explain the dearth of dwarf galaxies and the smoothness of galaxy core halos .
From this , all parameters of the scalar dark matter potential are completely determined .
The dark matter consists of an ultra-light particle , whose mass is m _ { \Phi } \simeq 1.1 \times 10 ^ { -23 } { eV } and all the success of the standard cold dark matter model is recovered .
This implies that a scalar field could also be a good candidate as the dark matter of the Universe .