Solar flares are the largest energy releasing events in the solar system, where the open magnetic field lines have reconnected and form the closed flare loops. During this process, rapid magnetic reconnection, the associated shock waves, and chromospheric evaporation are expected but not yet well understood. These processes are crucial for understanding similar features in stellar flares and other astrophysical jets. Here, we present a series of high-resolusion three-dimensional magnetohydrodynamics simulations for a typical solar eruption, due to loss of equilibrium for a pre-existing flux rope in the corona. Firstly, a complex evolution of plasmoids in the reconnection current sheet is witnessed in 3D, such as the splitting, merging and kinking processes. And the anisotropy of the turbulence shows a significant variation in the spectra with height. Secondly, the 3D Quasi-periodic fast propagating waves generated during the eruption are demonstrated to be composed of three distinct components: fast-mode shock, rarefaction wave and the transition region between them. The anisotropy of the 3D CME shock waves is responsible for the dome-like wave front observed in the extreme ultraviolet waves. Lastly, we found that normal slow shocks are recurrently formed after the collision between the post-reconnection downflows and evaporation flows in the flare loops, which subsequently propagate toward the chromosphere at speeds comparable to the evaporation flows. Our simulation and spectrum observation provide the reliable evidence to support the presence of the normal slow shocks on the leg of the flare loops, suggesting a significant advancement in the standard flare model framework.